Theoretical study of $\gamma$ Doradus pulsations in pre-main sequence stars

TL;DR

This paper theoretically investigates the existence and properties of $b3$ Doradus pulsations in pre-main sequence stars, deriving the instability strip and exploring how to distinguish PMS from MS pulsators through period spacing of gravity modes.

Contribution

It provides the first theoretical instability strip for PMS $b3$ Doradus stars and proposes a method to differentiate PMS from MS pulsators using period spacing analysis.

Findings

Derived the theoretical instability strip for PMS $b3$ Doradus stars.

Identified the potential of period spacing behavior to distinguish PMS from MS pulsators.

Explored pulsation properties across a range of stellar masses.

Abstract

The question of the existence of pre-main sequence (PMS) $\gamma$~Doradus ($\gamma$~Dor) has been raised by the observations of young clusters such as NGC~884 hosting $\gamma$~Dor members. We have explored the properties of $\gamma$~Dor type pulsations in a grid of PMS models covering the mass range $1.2 M_\odot < M_* < 2.5 M_\odot$ and we derive the theoretical instability strip (IS) for the PMS $\gamma$~Dor pulsators. We explore the possibility of distinguishing between PMS and MS $\gamma$~Dor by the behaviour of the period spacing of their high order $gravity$-modes ($g$-modes).